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On the unreasonable accuracy of the post-Newtonian approximation in gravitational-wave physics
- 1. Clifford Will Washington University Institute for Gravitation and the Cosmos Conference Penn State University, August 9-11, 2007 On the unreasonable accuracy of the post-Newtonian approximation in gravitational-wave physics
- 2. Interferometers Around The World LIGO Hanford 4&2 km LIGO Livingston 4 km GEO Hannover 600 m TAMA Tokyo 300 m Virgo Cascina 3 km
- 3. LISA: a space interferometer for 2018
- 8. DIRE: Direct integration of the relaxed Einstein equations Einstein’s Equations “ Relaxed” Einstein’s Equations
- 9. PN equations of motion for compact binaries B F S W B W W B = Blanchet, Damour, Iyer et al F = Futamase, Itoh S = Schäfer, Jaranowski W = WUGRAV
- 10. Gravitational energy flux for compact binaries W B W B W B B = Blanchet, Damour, Iyer et al F = Futamase, Itoh S = Schäfer, Jaranowski W = WUGRAV B B Wagoner & CW 76
- 12. The Binary Pulsar: Is strong gravity “effaced”? Discovery: 1974 Pulse period: 59 ms (16cps) Orbit period: 8 hours -2.4184(9) Orbit Decay (dP b /dt 10 -12 ) 4.2919(8) Pulsar Clock Shifts (ms) 4.226595(5) Periastron Shift (d /dt o /yr) Post-Keplerian 0.6171338(4) Eccentricity 0.322997448930(4) Orbit Period (days) 59.029997929613(7) Pulse Period (ms) Keplerian Value Parameter
- 13. m p = 1.4411(7) M sun m c = 1.3874(7) M sun PSR 1913+16: Concordance with GR
- 14. Decay of the orbit of PSR 1913+16 From Weisberg & Taylor (astro-ph/0407149)
- 17. Numerical Relativity meets PN Theory (NRm3PN)
- 19. How black holes get their kicks Favata, et al Getting a kick out of numerical relativity Centrella, et al A swift kick in the as trophysical compact object Boot, Foot, et al Recoiling from general relativists The Abhorrent Collaboration Total recoil: the maximum kick…. Gonzalez et al
- 21. Recoil velocity as a function of mass ratio X = 0.38 V max = 250 ± 50km/s V/c ≈ 0.043 X 2 Blanchet, Qusailah & CW (2005) X=1/10 V = 70 ± 15 km/s
- 22. Maximum recoil velocity: Range of Estimates 0 100 200 300 400 Favata, Hughes & Holtz (2004) Campanelli (Lazarus) (2005) Blanchet, Qusailah & CW (2005) Damour & Gopakumar (2006) Baker et al (2006)
- 23. Getting a kick from numerical relativity Baker et al (GSFC), gr-qc/0603204
- 27. “ Eccentric” orbits in relativistic systems. III 3PN ADM energy and angular momentum at apocenter
- 28. How well does the PN expansion converge?
- 30. Corotating Black Holes - Meudon Data
- 31. Corotating and Non-Spinning Binary Black Holes Caudill et al Caudill et al Tichy-Brügmann, Lazarus Cook-Pfeiffer, Caudill et al
- 32. Energy of Corotating Neutron Stars - Numerical vs. PN Simulations by Miller, Suen & WUGRAV
- 33. Energy of irrotational neutron stars - PN vs Meudon/Tokyo Data from Taniguchi & Gourgoulhon PRD 68, 124025 (2003) Diagnostic by Berti, Iyer & CMW (2007)
- 34. E b J Inferred eccentricities: irrotational neutron stars
- 35. BH - NS Initial Configurations Data from Taniguchi et al, gr-qc/0701110 Grandclement, gr-qc/0609044 [v5]
- 36. r ≈ 5M NRm3PN Comparing High-order PN with Numerical Waveforms Baker et al. gr-qc/0612024
- 37. r ≈ 4.6M NRm3PN Comparing High-order PN with Numerical Waveforms Hannam et al . arXiv:0706.1305
- 38. Reasonable vs. Unreasonable End of PN validity “ Best” numerical relativity